论文标题
对称能量对密集富含中子物质的声速和旋转分解的影响
Impact of Symmetry Energy on Sound Speed and Spinodal Decomposition in Dense Neutron-Rich Matter
论文作者
论文摘要
我们使用用于状态核方程（EO）的元模型及其参数受到天体物理观察和陆核实验的约束，我们检查了核EOS的影响，尤其是其对称能量\ ESYM对声音$ c^2_s（ρ）$的速度和关键密度$ρ_t$ c^2_s $ c^2_s $ panishe panish panish panish nish panish canse fanish panish panish panish的效果（这两种密集的富含中子的核这个物质与相对论重的沉重离子碰撞相关，而冷$ n+p+e+μ$在中子恒星中以$β$平衡为单位。与具有固定值的核酸物质不同，依赖密度依赖的同胞素谱$δ（ρ）$始终由$β$ quilibrium和电荷中性条件确定，$ c^2_s（ρ）$始终显示出$ c^2_s（ρ）$几乎总是显示出峰值，然后在$ρ_t$上消失。后者强烈取决于\ esym的高密度行为，如果表征高密度对称核物质（SNM）EOS的刚度的偏度参数$ J_0 $不超过其当前已知的最可能的价值，该价值的价值约为$ -190 $ -190 $ MEV，从最近的贝叶斯分析中的中子星星可观料分析中推断出来。此外，在具有核问题的饱和密度的两倍以上的密度降低的情况下，$ρ_T$的降低是$ρ_t$的降低的，则$ρ_T$明显低于\ esym消失的密度（表明Isospin-epareparation-epareparation-eareparation nocibalitionalitionbilitionalitionbility and Neutnobility and pure Netron Matteration and pure Neutron Matteration and Neutmon Star cores in Netmon Star cores in Netron Star cores in star cares sater cares satere care中的饱和密度降低了。
Using a meta model for nuclear Equation of State (EOS) with its parameters constrained by astrophysical observations and terrestrial nuclear experiments, we examine effects of nuclear EOS especially its symmetry energy \esym term on the speed of sound squared $C^2_s(ρ)$ and the critical density $ρ_t$ where $C^2_s(ρ_t)$ vanishes (indicating the onset of spinodal decomposition) in both dense neutron-rich nucleonic matter relevant for relativistic heavy-ion collisions and the cold $n+p+e+μ$ matter in neutron stars at $β$-equilibrium. Unlike in nucleonic matter with fixed values of the isospin asymmetry $δ$, in neutron stars with a density dependent isospin profile $δ(ρ)$ determined consistently by the $β$ equilibrium and charge neutrality conditions, the $C^2_s(ρ)$ almost always show a peak and then vanishes at $ρ_t$. The latter strongly depends on the high-density behavior of \esym if the skewness parameter $J_0$ characterizing the stiffness of high-density symmetric nuclear matter (SNM) EOS is not too far above its currently known most probable value of about $-190$ MeV inferred from recent Bayesian analyses of neutron star observables. Moreover, in the case of having a super-soft \esym that is decreasing with increasing density above about twice the saturation density of nuclear matter, the $ρ_t$ is significantly lower than the density where the \esym vanishes (indicating the onset of isospin-separation instability and pure neutron matter formation) in neutron star cores.
